Computer Science – Numerical Analysis
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ssrv...27..267d&link_type=abstract
(International Astronomical Union, Colloquium on Stellar Hydrodynamics, 58th, Los Alamos, N. Mex., Aug. 12-15, 1980.) Space Scie
Computer Science
Numerical Analysis
8
Dynamic Stability, Fission, Numerical Analysis, Polytropic Processes, Stellar Rotation, Angular Momentum, Computer Programs, Stellar Models
Scientific paper
A three-dimensional hydrodynamic computer code was used to study the nonlinear growth of nonaxisymmetric perturbations in rapidly rotating polytropes in an effort to understand the fate of dynamically unstable stars. It is shown that n = 3/2 and n = 1/2 polytropes are dynamically unstable to nonaxisymmetric perturbations if t is not less than about 0.30, in rough agreement with linear theory. Instead of fission as the direct end product of dynamic instability in rapidly rotating centrally condensed stars, it appears that a rapidly rotating star can, through gravitational torques, eject some high angular momentum material in its equatorial plane and settle down into a dynamically stable (lower t) configuration. The central object ends up as a stable triaxial star.
Durisen Richard H.
Tohline Joel E.
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